Weak lensing by large scale structure
Weak lensing by large scale structure
Weak lensing by large scale structure
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z=3<br />
z=1<br />
z=0<br />
Spot the difference...<br />
ΛCDM OCDM<br />
Different values for cosmological<br />
parameters lead to a different<br />
distribution of (dark) matter and a<br />
different evolution.<br />
The clustering properties of matter as a<br />
function of <strong>scale</strong> and redshift can be used<br />
as a tool to measure the cosmology!<br />
Kauffmann et al.
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